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The globular cluster luminosity function, specific globular clusterfrequency, S_N, specific globular cluster mass, T_MP, and globular cluster massfraction in dwarf elliptical galaxies are explored using the full 69 galaxysample of the HST WFPC2 Dwarf Elliptical Galaxy Snapshot Survey. The GCLFs ofthe dEs are well-represented with a t_5 function with a peak atM_{V,Z}^0(dE,HST) = -7.3 +/- 0.1. This is ~0.3 magnitudes fainter than the GCLFpeaks in giant spiral and elliptical galaxies, but the results are consistentwithin the uncertainties. The bright-end slope of the luminosity distributionhas a power-law form with slope alpha = -1.9 +/- 0.1. The trend of increasingS_N or T_MP with decreasing host galaxy luminosity is confirmed. The mean valuefor T_MP in dE,N galaxies is about a factor of two higher than the mean valuefor non-nucleated galaxies and the distributions of T_MP in dE,N and dE,noNgalaxies are statistically different. These data are combined with results fromthe literature for a wide range of galaxy types and environments. At low hostgalaxy masses the distribution of T_MP for dE,noN and dI galaxies are similar.This supports the idea that one pathway for forming dE,noN galaxies is by thestripping of dIs. The formation of nuclei and the larger values of T_MP in dE,Ngalaxies may be due to higher star formation rates and star cluster formationefficiencies due to interactions in galaxy cluster environments.

The Globular Cluster Luminosity Function and Specific Frequency in Dwarf Elliptical Galaxies